13 years of timing of PSR B1259−63

Wang, Na; Johnston, S.; Manchester, R. N.

doi:10.1111/j.1365-2966.2004.07806.x

Cited by 69 publications

(82 citation statements)

References 31 publications

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“…Three of them (No.1,3 and 4 in Fig.4) are with B or Be star companions (Kaspi et al 1994;Manchester et al 2001;Stairs, Manchester & Lyne 2001;Stairs et al 2003;Wang et al 2004). PSR J1638-4725 (No.2 in Fig.4) has a massive star as its companion (M c > 8.08M ⊙ ) which is in the main sequence stage.…”

Section: Type-i: Bpsrs With Massive Companionsmentioning

confidence: 99%

Binary pulsars in magnetic field versus spin period diagram

Yuanyue

Wang

Zhang

2013

Astrophys Space Sci

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We analyzed 186 binary pulsars (BPSRs) in the magnetic field versus spin period (B-P) diagram, where their relations to the millisecond pulsars (MSPs) can be clearly shown. Generally, both BPSRs and MSPs are believed to be recycled and spun-up in binary accreting phases, and evolved below the spin-up line setting by the Eddington accretion rate (Ṁ ≃10 18 g/s). It is noticed that most BPSRs are distributed around the spin-up line with mass accretion rateṀ = 10 16 g/s and almost all MSP samples lie above the spin-up line withṀ ∼ 10 15 g/s. Thus, we calculate that a minimum accretion rate (Ṁ ∼ 10 15 g/s) is required for the MSP formation, and physical reasons for this are proposed. In the B-P diagram, the positions of BPSRs and their relations to the binary parameters, such as the companion mass, orbital period and eccentricity, are illustrated and discussed. In addition, for the seven BPSRs located above the limit spin-up line, possible causes are suggested.

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Section: Type-i: Bpsrs With Massive Companionsmentioning

confidence: 99%

Binary pulsars in magnetic field versus spin period diagram

Yuanyue

Wang

Zhang

2013

Astrophys Space Sci

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“…The orbital phase of the binary system during the observation was 0.243, computed using the ephemerides in Wang, Johnston & Manchester (2004), and corresponds to 29.3 days after the periastron passage. Six antennas participated in the observations: ATCA (as a phased array), Ceduna, Hobart, Mopra, Parkes, and Tidbinbilla (we note that the data from Tidbinbilla could not be properly calibrated and were not included in the final data reduction).…”

Section: Lba Observations and Data Reductionmentioning

confidence: 99%

“…The truncation distance expands rapidly after periastron passage. Therefore we used the orbital solution of Wang, Johnston & Manchester (2004), a stellar mass of 31 M ⊙ (Negueruela et al 2011), and the typical neutron star mass of 1.4 M ⊙ to calculate the binary separation distance, r, as a function of time. The separation values range from 24.8 R ⋆ < r < 203.3 R ⋆ over the course of our observations.…”

Section: Evolution Of the Be Star Disk Mass And Size Based On The Hα mentioning

confidence: 99%

Multi-wavelength observations of the binary system PSR B1259−63/LS 2883 around the 2014 periastron passage

Chernyakova

Neronov

Soelen

et al. 2015

Mon. Not. R. Astron. Soc.

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We report on broad multi-wavelength observations of the 2010-2011 periastron passage of the γ-ray loud binary system PSR B1259−63. High resolution interferometric radio observations establish extended radio emission trailing the position of the pulsar. Observations with the Fermi Gamma-ray Space Telescope reveal GeV γ-ray flaring activity of the system, reaching the spin-down luminosity of the pulsar, around 30 days after periastron. There are no clear signatures of variability at radio, X-ray and TeV energies at the time of the GeV flare. Variability around periastron in the Hα emission line, can be interpreted as the gravitational interaction between the pulsar and the circumstellar disk. The equivalent width of the Hα grows from a few days before periastron until a few days later, and decreases again between 18 and 46 days after periastron. In near infrared we observe the similar decrease of the equivalent width of Brγ line between the 40th and 117th day after the periastron. For the idealized disk, the variability of the Hα line represents the variability of the mass and size of the disk. We discuss possible physical relations between the state of the disk and GeV emission under assumption that GeV flare is directly related to the decrease of the disk size.

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“…Both a dilute polar wind and a denser equatorial disc have been invoked to reconcile models for infrared, ultra-violet and optical observations (Waters et al 1988). Timing analysis of the PSR B1259-63 system shows that the disc of Be star is tilted with respect to the orbital plane (Wex et al 1998;Wang et al 2004). The properties of the radio emission ⋆ E-mail:Masha.Chernyakova@obs.unige.ch † M.Chernyakova is on leave from Astro Space Center of the P.N.…”

Section: Introductionmentioning

confidence: 99%

XMM-Newton observations of PSR B1259–63 near the 2004 periastron passage

et al. 2005

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PSR B1259-63 is in a highly eccentric 3.4 year orbit with a Be star and crosses the Be star disc twice per orbit, just prior to and just after periastron. Unpulsed radio, X-ray and gammaray emission observed from the binary system is thought to be due to the collision of pulsar wind with the wind of Be star. We present here the results of new XMM-Newton observations of the PSR B1259-63 system during the beginning of 2004 as the pulsar approached the disc of Be star. We combine these results with earlier unpublished X-ray data from BeppoSAX and XMM-Newton as well as with ASCA data. The detailed X-ray lightcurve of the system shows that the pulsar passes (twice per orbit) through a well-defined gaussian-profile disk with the half-opening angle (projected on the pulsar orbit plane) ∆θ disk ≃ 18.5• . The intersection of the disk middle plane with the pulsar orbital plane is inclined at θ disk ≃ 70• to the major axis of the pulsar orbit. Comparing the X-ray lightcurve to the TeV lightcurve of the the system we find that the increase of the TeV flux some 10-100 days after the periastron passage is unambiguously related to the disk passage. At the moment of entrance to the disk the Xray photon index hardens from Γ ≃ 1.8 up to Γ ≃ 1.2 before returning to the steeper value Γ 1.5. Such behaviour is not easily accounted for by the model in which the X-ray emission is synchrotron emission from the shocked pulsar wind. We argue that the observed hardening of the X-ray spectrum is due to the inverse Compton or bremsstrahlung emission from 10-100 MeV electrons responsible for the radio synchrotron emission.

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13 years of timing of PSR B1259−63

Cited by 69 publications

References 31 publications

Binary pulsars in magnetic field versus spin period diagram

Binary pulsars in magnetic field versus spin period diagram

Multi-wavelength observations of the binary system PSR B1259−63/LS 2883 around the 2014 periastron passage

XMM-Newton observations of PSR B1259–63 near the 2004 periastron passage

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